標(biāo)題: Titlebook: Galaxy Evolution in Groups and Clusters; A JENAM 2002 Worksho Catarina Lobo,Margarida Serote Roos,Andrea Biviano Book 2003 Springer Science [打印本頁] 作者: 不要提吃飯 時間: 2025-3-21 19:18
書目名稱Galaxy Evolution in Groups and Clusters影響因子(影響力)
書目名稱Galaxy Evolution in Groups and Clusters影響因子(影響力)學(xué)科排名
書目名稱Galaxy Evolution in Groups and Clusters網(wǎng)絡(luò)公開度
書目名稱Galaxy Evolution in Groups and Clusters網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Galaxy Evolution in Groups and Clusters被引頻次
書目名稱Galaxy Evolution in Groups and Clusters被引頻次學(xué)科排名
書目名稱Galaxy Evolution in Groups and Clusters年度引用
書目名稱Galaxy Evolution in Groups and Clusters年度引用學(xué)科排名
書目名稱Galaxy Evolution in Groups and Clusters讀者反饋
書目名稱Galaxy Evolution in Groups and Clusters讀者反饋學(xué)科排名
作者: chondromalacia 時間: 2025-3-21 23:41
Quantitative Study of Galaxy Morphology Release (SDSS EDR) galaxies of known redshift and brighter than r=16. The bulge-to-disk (B/D) luminosity ratios can be combined with an estimate of the galaxy’s local environment to address a number of key issues that are central to our understanding of galaxy formation:作者: subacute 時間: 2025-3-22 00:23
Characteristics of Meat Demand in GreeceWe derive the blue fraction for a sample of . -selected galaxies in 25 clusters at 0.15 < . < 0.92. We find a much smaller blue fraction and weaker trend with redshift than measured in optically selected samples. We suggest that the Butcher-Oemler effect is primarily due to star fonning low luminosity galaxies.作者: –DOX 時間: 2025-3-22 07:10
The , -Selected Butcher-Oemler EffectWe derive the blue fraction for a sample of . -selected galaxies in 25 clusters at 0.15 < . < 0.92. We find a much smaller blue fraction and weaker trend with redshift than measured in optically selected samples. We suggest that the Butcher-Oemler effect is primarily due to star fonning low luminosity galaxies.作者: 使厭惡 時間: 2025-3-22 12:33 作者: diathermy 時間: 2025-3-22 16:58 作者: diathermy 時間: 2025-3-22 20:14
An Object Model for Geologic Map Informationlaxy evolution. This review discusses some of the recent observations of moderate to high redshift clusters. A consistent picture of galaxy evolution in clusters appears to be emerging, which includes a population of galaxies which formed early in the cluster history, as well as field galaxies which作者: amputation 時間: 2025-3-23 01:03 作者: Spinal-Tap 時間: 2025-3-23 03:33 作者: Basilar-Artery 時間: 2025-3-23 07:26
James A. Rodger,James A. Georgethe Nearby Optical Galaxy sample, by means of hierarchical and percolation ‘friends-of-friends’ methods. We find that earlier-type (brighter) galaxies are more clustered and lie closer to the group centers, both in position and in velocity, than later-type (fainter) galaxies. Spatial segregations ar作者: 頌揚本人 時間: 2025-3-23 12:25 作者: CRATE 時間: 2025-3-23 16:24
G. R. Gandhe,V. S. Kulkarni,Y. M. Ghugaleir use as cosmological probes. BCGs form a unique galaxy population. They are located near the gravitational centre of galaxy clusters and are the most massive galaxies in the universe, being some 10 times more luminous than L. systems. Historically, BCGs have been credited with small intrinsic dis作者: capillaries 時間: 2025-3-23 18:03 作者: Rejuvenate 時間: 2025-3-23 22:45
Raghu Prakash,Vikram Jayaram,Ashok Saxenaface brightness profiles of BCGs out to large radii is critical for understanding the processes driving their formation. The form of the profiles yields information about the current dynamical state, constrains the accretion history of these galaxies, and places limits on any radially symmetric comp作者: MURAL 時間: 2025-3-24 05:42
Machi Zawidzki,?ukasz Jankowski Release (SDSS EDR) galaxies of known redshift and brighter than r=16. The bulge-to-disk (B/D) luminosity ratios can be combined with an estimate of the galaxy’s local environment to address a number of key issues that are central to our understanding of galaxy formation:作者: 嚴(yán)厲批評 時間: 2025-3-24 07:11 作者: Antimicrobial 時間: 2025-3-24 12:28 作者: Debark 時間: 2025-3-24 17:42
Takehiko Ishiguro,Koji Kajimura function is not universal, but seems to be strongly dependent upon environment. In this paper we describe an automated procedure for detecting and measuring very Low Surface Brightness (LSB) features in deep CCD data. We apply this procedure to large area CCD survey fields of the Virgo cluster and 作者: Legion 時間: 2025-3-24 22:13
High-Tc Thin-Film Microelectronics(A0952 + 69) and Garland using HST/WFPC2 images of these galaxies. We construct a library of synthetic Colour-Magnitude Diagrams (CMDs) based on theoretical isochrones and data-derived determinations of photometric errors. These synthetic CMDs were combined linearly and ..-compared to observed photo作者: 磨坊 時間: 2025-3-25 01:09 作者: 我吃花盤旋 時間: 2025-3-25 03:47 作者: 手段 時間: 2025-3-25 08:42
Book 2003ok, intended primarily to researchers in the field, particular emphasis is given to the recent impressive progress in the field, on important new results, and on the future prospects and open questions to be tackled.作者: 陳列 時間: 2025-3-25 12:05
In this book, intended primarily to researchers in the field, particular emphasis is given to the recent impressive progress in the field, on important new results, and on the future prospects and open questions to be tackled.978-94-010-3975-8978-94-010-0107-6作者: 寬大 時間: 2025-3-25 16:02 作者: Flatter 時間: 2025-3-25 21:27 作者: Generalize 時間: 2025-3-26 01:46
Souradip Dasgupta,Tuhin Khan,Anindya Dattaht ellipticals is probably affected by dissipative processes which invalidate the use of the collisionless Jeans equation. The equilibrium solution found for the early-spirals implies them to move on nearly-isotropic orbits. Late-spirals are instead found to be on mildly radial orbits, with the radi作者: 變形 時間: 2025-3-26 07:21 作者: Precursor 時間: 2025-3-26 09:31
Raghu Prakash,Vikram Jayaram,Ashok Saxenaerally are best fit using two-component models consisting of inner and outer Sersic profiles. In this proceeding we present the preliminary results of our analysis and discuss implications for current models of BCG formation.作者: PAC 時間: 2025-3-26 15:28 作者: 首創(chuàng)精神 時間: 2025-3-26 17:23
Advances in Superconductivity IVture, the dwarf elliptical halo contents, up to 99% of the original dwarf luminosity, contribute a significant fraction of the populations of intergalactic stars, globulars, and gas in galaxy clusters.作者: 官僚統(tǒng)治 時間: 2025-3-26 22:06
Galaxy Evolution in Clusterss, perhaps because of the recent merging history of the clusters. We also present a recent analysis of population gradients in clusters which suggests that the observed evolution in cluster populations is consistent with a scenario where changing infall rates drive the fraction of star forming galax作者: 處理 時間: 2025-3-27 02:13
The Properties of the Galaxies in the Enacs Clusters, and the Relation Between Spirals and S0 Galaxithe early spirals (Sa-Sb), and the late spirals (including the emission-line galaxies). We also study the morphology-density relation, and we find that the segregation of the late spirals is driven mostly by global factors, while the segregation of Es, S0s and early spirals is driven mostly by local作者: 吹牛大王 時間: 2025-3-27 08:04
The Orbits of Cluster Galaxy Populations as Evolutionary Constraintsht ellipticals is probably affected by dissipative processes which invalidate the use of the collisionless Jeans equation. The equilibrium solution found for the early-spirals implies them to move on nearly-isotropic orbits. Late-spirals are instead found to be on mildly radial orbits, with the radi作者: 抱怨 時間: 2025-3-27 11:15 作者: Buttress 時間: 2025-3-27 14:28 作者: 遣返回國 時間: 2025-3-27 21:34
Dwarf LSB Galaxies and their Environment: The Virgo Cluster, The URSA Major Cluster, Isolated Galaxiy contribute significantly to the mass in galaxies if they have large mass-to-light ratios similar to those recently measured for Local Group dwarf galaxies..By a comparison with different environments, the Virgo Cluster seems to be highly ‘dwarf rich’ if considering the dwarf to giant ratio or its 作者: FIR 時間: 2025-3-28 00:37
Galaxy Threshing and Ultra-Compact Dwarfs in the Fornax Clusterture, the dwarf elliptical halo contents, up to 99% of the original dwarf luminosity, contribute a significant fraction of the populations of intergalactic stars, globulars, and gas in galaxy clusters.作者: 天真 時間: 2025-3-28 04:29 作者: 逃避現(xiàn)實 時間: 2025-3-28 09:39 作者: bacteria 時間: 2025-3-28 13:22 作者: Toxoid-Vaccines 時間: 2025-3-28 18:03
The Fundamental Plane of E Galaxies in Compact Groupse position of II compact group galaxies in the Fundamental Plane to that of a large and homogeneous sample of elliptical galaxies (Burstein et aI., 1987). We find that little or no significant difference exists, as far as the Fundamental Plane is concerned, between ellipticals in compact groups and their counterparts in other environments.作者: Bombast 時間: 2025-3-28 21:02 作者: Spartan 時間: 2025-3-29 02:02
H. Kasahara,S. Akita,T. Ishikawa,T. Tanaka. While concluding, we present, as well, future prospects on how to measure distances to dwarfs using the surface brightness fluctuation method so as to increase the number of confirmed dwarf member galaxies in more distant clusters.作者: Ejaculate 時間: 2025-3-29 04:44
High-Tc Thin-Film Microelectronicsormed out of material from metal-poor outer part of the giant spiral galaxy M81 after tidal interaction about 200 Myr ago. However, this suggestion requires significantly more deep color-magnitude diagrams to be sure with the scenario of the galaxy evolution.作者: 兵團(tuán) 時間: 2025-3-29 11:15
Morphology and Luminosity Segregations in Galaxy Groupsbers), and are strengthened by the detection of segregation in both hierarchical and percolation catalogs. Luminosity segregation is shown to be independent of morphology segregation. Our conclusions agree with a continuum of segregation properties of galaxies in systems, from low-mass groups to massive clusters.作者: Connotation 時間: 2025-3-29 13:07 作者: output 時間: 2025-3-29 19:05 作者: 顯而易見 時間: 2025-3-29 20:15 作者: optional 時間: 2025-3-30 03:21 作者: STAT 時間: 2025-3-30 05:28 作者: Morose 時間: 2025-3-30 11:02
The Evolutionary Status of Early-Type Galaxies in Abell 2390ubsample of 14 galaxies with morphological and structural parameters from HST, we also investigate the evolution of the Kormendy relation and the Fundamental Plane. We find a mild luminosity evolution of the early-type galaxies in Abell 2390: our objects are on average brighter by .. ～ 0.4 mag.作者: Palpitation 時間: 2025-3-30 12:34 作者: etidronate 時間: 2025-3-30 20:02 作者: 離開真充足 時間: 2025-3-30 20:51
The Orbits of Cluster Galaxy Populations as Evolutionary Constraints(ENACS). We use ellipticals and S0s as tracers of the cluster potential, and solve the Jeans equation assuming isotropic orbits. Such an assumption is justified by the analysis of the shape of the velocity distribution of ellipticals and S0s. We find that the cluster mass profile is consistent with 作者: majestic 時間: 2025-3-31 03:40
Morphology and Luminosity Segregations in Galaxy Groupsthe Nearby Optical Galaxy sample, by means of hierarchical and percolation ‘friends-of-friends’ methods. We find that earlier-type (brighter) galaxies are more clustered and lie closer to the group centers, both in position and in velocity, than later-type (fainter) galaxies. Spatial segregations ar作者: Scleroderma 時間: 2025-3-31 08:03
The Velocity Dispersion In The X-Ray Scaling Lawsand the optical velocity dispersion σ. We obtained redshifts for the fainter members of these groups. We find that X-ray bright groups have more members and higher velocity dispersions on average. Using the fainter group members and Monte Carlo tests, we define the number of group members required t作者: 帶來 時間: 2025-3-31 12:07
The Evolution of Brightest Cluster Galaxieseir use as cosmological probes. BCGs form a unique galaxy population. They are located near the gravitational centre of galaxy clusters and are the most massive galaxies in the universe, being some 10 times more luminous than L. systems. Historically, BCGs have been credited with small intrinsic dis作者: 制度 時間: 2025-3-31 17:05 作者: 繼而發(fā)生 時間: 2025-3-31 18:38
Structural Properties of Brightest Cluster Galaxiesface brightness profiles of BCGs out to large radii is critical for understanding the processes driving their formation. The form of the profiles yields information about the current dynamical state, constrains the accretion history of these galaxies, and places limits on any radially symmetric comp
